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Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS) Xavier Barcons On behalf of the AXIS/XMS/SSC team.

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Presentation on theme: "Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS) Xavier Barcons On behalf of the AXIS/XMS/SSC team."— Presentation transcript:

1 Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS) Xavier Barcons On behalf of the AXIS/XMS/SSC team

2 El EscorialThe X-ray Universe 2005 Index lThe role of medium sensitivity surveys lThe XMS survey lThe content of the XMS survey lTips for statistical identifications lOutlook and future work

3 El EscorialThe X-ray Universe 2005 The role of Medium Surveys lBridge between most popular deep surveys and surveys of the local Universe lThe average XMM-Newton observation (10-20 ks of GTI) is a Medium Sensitivity Survey: *The 2XMM catalogue will be a huge MSS lThe bulk of the cosmic X-ray background resides at intermediate X-ray fluxes (~ erg cm -2 s -1 )

4 El EscorialThe X-ray Universe 2005 Relative contribution to XRB per flux decade  S dN(S)/d log S

5 El EscorialThe X-ray Universe 2005 Fraction of XRB resolved by X-ray surveys Deep XMS BSS The XMS resolves ~50% of the keV X-ray background

6 The XMS survey and its optical identification

7 El EscorialThe X-ray Universe 2005 Definition of the XMS sample l25 XMM-Newton target fields: *Galactic latitude |b|>20 deg *X-ray observations with EPIC-pn detector in FULL-FRAME-MODE *~Avoided fields with bright and/or extended targets *Good time intervals > 10 ksec *Available early on in the mission lUsing SAS v6.1.1 to produce final source list and products: *Exposure and background maps *Source detection *Spectra and calibration matrices lAreas around target + OOT+ near the pn CCD gaps excluded lOwn empirical sentitivity maps from detected source parameters l284 sources with keV flux > erg cm -2 s -1 lVery detailed source screening NGC4291 Mrk 205

8 El EscorialThe X-ray Universe 2005 Statistics of XMS fields FieldGTI#g’r’i’ A  A  B  B  Cl  Cl  Eq Peg 1214 G133_21811 G133_1208 HD  IRAS  LBQS  UZ Lib 237Mkn  Mkn32313 MS  MS  PB  PHL  PKS  PKS  S  SDS14313 SDS2419 SDS3146

9 El EscorialThe X-ray Universe 2005 Optical identification of XMS lOptical imaging: g’,r’,i’ and more to r’~23-24 mag lReliable & unique candidate counterpart in r’/i’ for virtually all sources (< 5” or < 5  ) lOptical spectroscopy *50% from AXIS programme (WHT, TNG, NOT): multi-fibre and long-slit spectroscopy *20% from Calar Alto/3.5m long-slit spectroscopy *15% from VLT/FORS2 long-slit spectroscopy *A few from AAT/2dF, SUBARU/FOCAS, and others lPreliminary results from 2 XMM-Newton fields (~30 sources) in Barcons et al (2002)

10 El EscorialThe X-ray Universe 2005 XMS Identification status l25 XMM fields lXID: keV lS XID >2  cgs lΩ=3.3 deg 2

11 The content of the XMS Identification breakdown Remaining incompleteness & biases Towards the X-ray luminosity function

12 El EscorialThe X-ray Universe 2005 Breakdown of identified sources in the XMS ClassNumber% Broad-Line AGN Narrow Line Galaxies3715 Absorption Line Galaxies 84 Stars187 BL Lac 10

13 El EscorialThe X-ray Universe 2005 Fluxes and redshifts

14 El EscorialThe X-ray Universe 2005 Incompleteness and remaining biases

15 El EscorialThe X-ray Universe 2005 Redshift distribution

16 El EscorialThe X-ray Universe 2005 QSO-2s S( )= erg cm -2 s -1 z=0.711 L X = erg s -1 Absorbed:  =0.55

17 El EscorialThe X-ray Universe 2005 The L-z plane and the X-ray Luminosity Function Deep Surveys Bright Source Survey Unfortunately, photo-z’s do not work with our limited colour information

18 El EscorialThe X-ray Universe 2005 Source counts S b =  cgs Γu= Γd= See poster G.2 for more details

19 El EscorialThe X-ray Universe 2005 X-ray spectral properties of AGN lSpectra of individual sources well matched to unified model, but with exceptions (Mateos et al 2005) lX-ray spectral templates: de-redshifted average spectra (see poster E.11 by Corral et al) ? ?

20 Tips on statistical identification

21 El EscorialThe X-ray Universe 2005 Statistical identification lProbabilistic classification of X-ray sources, based on: *X-ray colours *Optical colours *X-ray to optical flux ratios *X-ray and/or optical morphology lLarge parameter space: start with “preliminary inspection” (fishing expedition), later apply mathematical tools (PCA, ANNs, etc.)

22 El EscorialThe X-ray Universe 2005 HR 2 =(H-S)/(H+S) H= keV S= keV 100% Stars >75% ALG 100% NELG >80% NELG >60% NELG >50% NELG >85% BLAGN

23 El EscorialThe X-ray Universe 2005 Optical colour-colour diagrams SDSS QSOs SDSS Early-type galaxies 50% NELGs 50% “red” BLAGNs 95% BLAGNs

24 El EscorialThe X-ray Universe 2005 Optical vs X-ray colours Red & Soft ALG Red & Hard NELGs Blue BLAGN

25 El EscorialThe X-ray Universe 2005 Obscuration/reddening

26 El EscorialThe X-ray Universe 2005 Obscuration/reddening

27 El EscorialThe X-ray Universe 2005 Tips for statistical identifications lSources with log (f X /f opt )<-1.5 are invariably stars lOptically blue objects are 95% BLAGN lOptically red objects include both broad-line and narrow line AGN lRed & soft galaxies do not have emission lines lRed & hard galaxies have narrow emission lines lThere is a large patch of parameter space shared by both broad and narrow line AGN.

28 El EscorialThe X-ray Universe 2005 Outlook and future work lSpectroscopic identification of remaining 15% objects needed (photo-z’s do not work) lCombine with Bright and Deep Surveys to compute AGN X-ray luminosity function and evolution lCompute Accretion power as a function of z, both for absorbed and unabsorbed sources lExplore larger sample (XMM/2dF) in the search for statistical identification handles lApply statistical identification to 2XMM catalogue

29 El EscorialThe X-ray Universe 2005 Thanks to: lFrancisco Carrera lMaite Ceballos lSilvia Mateos lAmalia Corral lFrancesca Panessa lJacobo Ebrero lMat Page lAxel Schwope lMike Watson lRoberto Della Ceca lJonathan Tedds lTommaso Maccacaro lAnd many more…


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